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A. Treves, L. Maraschi, M. Abramowicz's Accretion: A collection of influential papers PDF

By A. Treves, L. Maraschi, M. Abramowicz

ISBN-10: 9810200773

ISBN-13: 9789810200770

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Details of the stream lines in the vicinity of L\ are given by Lubow & Shu (1975). The stream leaving L\ has a core that is denser than the outer regions; the density profile should be approximately Gaussian. 7) where Q is the effective cross-section of the stream, pLl is the density at L\, averaged over the cross-section and cs is the similarly averaged isothermal sound velocity. 3 Mass flow through the inner Lagrangian point. From Pringle (1985). Mass Transfer 35 An approximate estimate of the radius W{= Q1/2/TT1/2) of the stream can be obtained by requiring that cs exceed the escape velocity from the secondary.

There is a third Lagrangian point, L3, on the opposite side of the system from Li. In order to find an approximate spherical stellar model for a Roche lobe-filling star, appeal is often made to the volume radius RL(2) of the Roche lobe. Computations have been made by Kopal (1959), Plavec & Kratochvil (1964) and Eggleton (1983a). 1. 1. Approximate Formulae involving the Roche Lobe. 1. 4056)-! 4c) 2. 49#2/3 +ln(l + q1/3) ! 3 < ? 5c) accurate to better than 1% 3. 2

1. There is a third Lagrangian point, L3, on the opposite side of the system from Li. In order to find an approximate spherical stellar model for a Roche lobe-filling star, appeal is often made to the volume radius RL(2) of the Roche lobe. Computations have been made by Kopal (1959), Plavec & Kratochvil (1964) and Eggleton (1983a). 1. 1. Approximate Formulae involving the Roche Lobe. 1. 4056)-! 4c) 2. 49#2/3 +ln(l + q1/3) ! 3 < ? 5c) accurate to better than 1% 3. 2

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Accretion: A collection of influential papers by A. Treves, L. Maraschi, M. Abramowicz


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